Novae and Accreting WDs as SN Ia Progenitors

Mariko Kato (Keio Univ.)

U Sco

2

outline

candidates of SN Ia progenitoroptically thick wind theory of nova outbursthow to find massive WDsVery massive WDs ; U Sco, RS Oph, V445 Pupposition in binary evolution scenarios (SD)RX J0523-69 : accretion wind evolution

comments on binary evolution scenarios to type Ia SN

3

nova evolution

All novae undergosupersoft

X-ray stage

Wind mass losscontinuously occurs

supersoftX-ray

UV

Optical

4

Optically thick wind theory

The unique method to calculate nova light-curvequasi-evolution: sequence of steady-state solutionsSolve equations of motion, continuity, diffusion, energy conservation

obtain accurate mass-loss rate, Tph, Lphlight curve :optical & IR: free-free emission

UV 1455A & X-ray: blackbody emission

Kato & Hachisu (1994), Hachisu & Kato (2006)

mass loss: continuum radiation-driven windFriedjung (1966)

5

The envelope structure

wind is driven by radiation-pressuregradient

not line-driven

photosphere

OPAL opacity Iglesias & Rogers (1991)

.

Caution:DD papers use old opacityIben, Tutukov, Yungelson

Accelerate strong windsChange in structure and mass-loss rate

Kato & Hachisu (1994)

7

Nova in HR diagram

optically thick wind

Supersoft X-ray wind

8

Theoretical Light Curve of Nova

Dependence of WD mass

optical

0.6 Mo1.2 M

o

9

V1974 Cyg: light curve fittingdetermine WD mass

Hachisu

& Kato(2005,2006)

X-ray: ROSAT : Orio

et al. (2001), Shanley

et al (1995)

UV IUE 1455 Å continuum:

Cassatella, Altamore, Gonzalez-Riestra

(2002)

1.0 ±0.05

Mo

10

WD Mass determined by light curve fittingclassical nova

V1500 Cyg (1.15 Mo), V1668 Cyg (0.95 Mo), OS And (1.0 Mo)V1974 Cyg (1.0 Mo), V838 Her (1.35 Mo), V351 Pup (1.05 Mo)GK Per (1.15 Mo), V2491 Cyg (1.3 Mo), V693 CrA ( 1.3 Mo)V1493 Aql (1.15 Mo), V2362 Cyg (0.7 Mo) , PU Vul (0.6 Mo)V2361 Cyg (1.05 Mo), V382 Nor (1.15 Mo), V5115 Sgr (1.2Mo) V378 Ser (0.7 Mo), V5116 Sgr (0.9 Mo), V1188 Sco(1.25 Mo)V1047 Cen (0.7 Mo), V476 Sct (0.95 Mo), V663 Aql (0.95 Mo)V477 Sct (1.3 Mo), V598 Pup (1.28Mo), V382 Vel (1.2Mo)V4743 Sgr (1.15Mo), V1281Sco (1.1 Mo), V597 Pup (1.1Mo)V2467 Cyg (1.0 Mo), V5116 Sgr (1.07Mo), V574 Pup (1.05Mo)V458 Vul (0.93Mo)

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Recurrent nova

U Sco (1.37 Mo ) Hachisu et al (2000) ApJLV394 CrA (1.37 Mo ) HK (2000, 2001) ApJLMC1990#2 (1.37Mo)T CrB (1.37 Mo) HK(2001) ApJ,558,323RS Oph (1.35 Mo) Hachisu et al. (2006, 2007)V745 Sco (1.35 Mo) HK (2001)V3890 Sgr (1.35 Mo) HK(2001)CI Aql (> 1.2 Mo) T Pyx (> 1.2 Mo)

Type Ia supernova candidates

RS Oph

T CrB

V394 CrA

U Sco

12

U Sco : Recurrent nova

Model: WD envelope+ irradiated Disk

+ irradiated companion(Hachisu et al. 2000)

Porb =1.23 d

1863,1906,1936,1979,1987,1999, 2010(43) (30) (43) (8) (12) (11)

Hachisu et al. (2000)

13

MWD ~1.37 MoPorb =1.23 d, i =80 degMcomp ~1.5 Moaccreted matter= 3x10-6 Mo (12 yr)mean accretion rate =3x10-7 Mo/yrejected matter = 1.8x10-6 Monet growth rate =1.0x10-7 Mo/yr (40 %)Candidate of Type Ia SN

U Sco : Recurrent nova

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V838 Her (1991)

Kato, Hachisu & Cassatella (2009) 704,1676

1.35 Mo

for X=0.55, O=0.03, Ne=0.07, Z=0.02

WD mass: 1.33 Mo1.35 Mo1.37 Mo

15

U Sco vs. V838 HerU Scorecurrent nova~1.38 MoMWD

V838 HerClassical nova~1.35 MoMWD

Very similar light curves

UV 1455A

optical

RN

CN

16

RN CNCO/ONeMg-richEjecta :

Recurrent nova and classical nova

WD

Solar abundance

MWD MWD

WDHe

SN Ia : initial and final state of binary

V838 Her

symbiotic channel

sss channel

Hachisu & Kato, Nomoto(2008) ApJL

Outburst: 1898,1933, 1958, 1967, 1985, 2006 Porb : 457 days (Fekel et al. 2000) i : ~30-40 °

RG : M0 (Anupama & Mikolajewska 1999) MIII (Evans et al. 1988)

well observed : radio ~ X-ray

RS Oph (Recurrent Nova)

RS Oph: 2006 outburst

optical: Hachisu et al. 2006 ApJLX-ray :Hachisu et al. 2007 ApJL

supersoftX-rays

y-mag

WD

hot He layer(heat reservoir)

H

20

Light curve model

Hachisu et al (2006,2007)

model: WD + disk + companionWD: free-free emissiondisk : irradiated (local TBB)companion : irradiated

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RS Oph : summary

WD mass : 1.35 ± 0.01 Mocomposition: X=0.2-0.4distance : 1.3 – 1.7 kpcaccreted mass: 4.x10-6 Mo (in 21 yrs)ejected mass: (2-2.8) x10-6 Mo (50-70%)remaining mass: (1.2-2) x10-6 Mo (30-50%)mean accretion rate: 2. x10-7 Mo/yr

WD mass: net growth rate (0.6-1) x10-7 Mo/yr

candidate of type Ia SN progenitor

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RS Oph

MWD ～ 1.35 MoNo metal rich

Hachisu et al. (2006, 2007)

V2491 Cyg

MWD ~ 1.3 Mometal rich

Hachisu & Kato (2009)

RS Oph vs. V2491 CygSimilar in optical, but very different in X-rays

RN

CN

SN Ia : initial and final state of binary

V838 HerV2491 Cyg GK Per RS Oph

sss channel

symbiotic channel

V445 Pup (2000) a He nova

• no H lines• strong emission lines C, Na, Fe,Ti, Cr, Si, Mg, etc.• P Cyg profile•resemble to slow classical novae => nova

Iijima & Nakanishi (2008) A&ApHe nova: He burnig

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V445 Pup : summary

WD mass : 1.35 – 1.38 MoDistance : 4-8 kpcWD mass : growth rate : ~ 50 % Candidate of type Ia SN progenitor

Kato et al (2008) ApJ, 684,1366

26

RX J0513-69 (LMC SSS)optical high & low statesupersoft X-ray; only in optical low state

supersoft X-ray

Cowley et al. (2002) AJ 124, 2233

Schaeidt et al (1993)Reinsch et al (1996)Southwell et al （1996)McGowan et al. (2005)Burwitz et al. (2008)

27

Model

.

winds

wind stops

mass accretionmakes a spray

disk and companionare spattered

by the wind

mass transferstops

companionsurface is stripped

Macc > Mcr ~0.75x10-6(MWD/Mo -0.4) Mo/yr → Winds・ ・

optical: brightno X-ray

optical: darkX-ray

Accretion wind

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limit cycle of the light curve

.

wind phase

envelope expands &large disk

no mass accretiononto WD

mass accretionstarts

windstops

mass transferfrom companion

disk flare up

supported by XMM observationMcGowan et al.(2005)

Hachisu & Kato, 2003, ApJ,590,445

29RX J0513 is a SN Ia progenitor

(time averaged)

RX J0513-69

MWD =1.2-1.3 Mo

Hachisu & Kato (2003) ApJ,590,445

Net growth rate

30

Net growth rate

V Sge (galactic SSS)

V Sge is a SN Ia progenitor

(time averaged)

Hachisu & Kato (2003) ApJ, 598,527

MWD = 1.2-1.3 Mo

SN Ia : initial and final state of binary

V838 HerV2491 Cyg GK Per RS Oph

RX J0523

V Sge

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Symbiotic channel in SD scenario

Hachisu et al 1999, ApJ

zero age

super-windfrom AGB star

commonenvelope-like

evolution

AGB

M1=4-9 MoM2=0.9-3 Moa=1500-30000 Ro

M1=0.9-1.2 MoM2=0.9-3 Moa=40-400 RoP=300-800 day

CO WD + MS

strong wind andmass stripping

from RG

SN Ia explosion

Recurrent novaRS Oph, T CrB

Recurrent novaRS Oph, T CrB

Accretionwind evolution

(original DD scenario)common envelope evolution

WD + WD

33Hachisu & Kato 2003

zero age

unstable mass

transfer

common envelope

He masstransfer

He rich envelope

of secondary

mass transfer

Accretion Wind

evolution

wind stops

SN Ia

SSX sourceRX J0513,V SgeSSX sourceRX J0513,V Sge

Recurrent novaU Sco, V394 CrA

Recurrent novaU Sco, V394 CrA

SSS channel in SD scenario

(original DD scenario)common envelope evolution

merging

Response of Accreting WDs

Hachisu & Kato (2001)ApJ 558,323

Nova

MWD (Mo )

mas

s ac

cret

ion

rate

in DD scenariocommon envelope evolution

double WDs/ merging

SSS source

Nova

Accretion wind evolutionWD becomes massive

AccretionWind

35

Nova & SN people need more communication

Physics of accreting WDs, widely accepted in nova, is not known in SN community

nova supernova

Starrfield et al. (2004) ApJ, 612,L53 “surface H burning”

Wrong resultstoo small mesh pointtoo large time-step

Nomoto, Saio, Kato,& Hachisu (2007) ApJ, 663,1269

=10-9 - 8x10-7 Mo /yr

He “found ”No novae occur

SN IaNova

MWD (Mo )

H-burningis stable !

37

King et al. (2003) MNRAS, 341, L35 A new evolutionary channel for type Ia SN “Dwarf nova causes steady H-burning”

WD grows SNMWD (Mo )

Dwarf nova outburst

temporal increase

H steadily burns (no loss)

Macc. (disk instability)

However, H does not ignite during dwarf nova outburst

Shell flash occurs ifMenv > Mig(Pc > Pcr )

much larger than Mdisk

see also Hachisu et al (2010) ApJL

Necessary condition of shell flashis not for the mass-accretion rate

but for the envelope mass

H burning is unstable Nova MWD decreases

39

papers adopted King et al.’ ideapopulation synthesisduring dwarf nova outburst: 100 xXu & Li (2009) AAp, 495,243Wang & Han (2010) RAA, 10, 235Wang, Li & Han (2010) MNRAS, 401, 2729

always 100xMeng & Yang (2010) ApJ, 710,1310

These results have no astrophysical meaning

Macc.

Macc.

WDs evolve along with “steady burning zone” ?

many papers overestimate SSS phase,e.g.Di Stefano (except recent)YungelsonGilfanov & Bogdan (2010) Nature,463,924MWD (Mo )

ignore binary evolution

papers

decreasesHachisu et al. (1999)

ApJ, 519, 314ApJ, 522, 487

Macc.

to estimate number of SSS

41

Yungelson (2005) AIPC, 797,1 Tutukov & Fedorova (2007) AR,51,291Podsiadlowski (2010) AN 331,218

DD-merger is a bright supersoft X-ray sourceL ~1038 erg/s, t ~ 105 yrT ~ (0.5-1)x 106K

DD scenarios predict SSS

DD scenario contains no supersoft X-ray source ?

overproduction problem of SSS

42

RS Oph：1.35 Mo

T CrB 1.37 Mo

V394 CrA：

1.37 MoU Sco：

1.37 Mo

Thank youThank you

Novae and Accreting WDs �as SN Ia Progenitorsoutlinenova evolutionOptically thick wind theory The envelope structure OPAL opacity Iglesias & Rogers (1991)Nova in HR diagramTheoretical Light Curve of NovaV1974 Cyg: light curve fittingWD Mass determined by light curve fittingRecurrent novaU Sco : Recurrent novaU Sco : Recurrent novaV838 Her (1991)U Sco vs. V838 HerEjecta :　�　　　　SN Ia : initial and final state of binaryOutburst: 1898,1933, 1958, 1967, 1985, 2006�Porb : 457 days (Fekel et al. 2000) � i : ~30-40 °�RG :　M0 (Anupama & Mikolajewska 1999) � MIII (Evans et al. 1988) �well observed : radio ~ X-rayRS Oph: 2006 outburstLight curve model RS Oph : summaryRS Oph vs. V2491 CygSN Ia : initial and final state of binaryV445 Pup (2000) �a He novaV445 Pup :� summary RX J0513-69 (LMC SSS)Modellimit cycle of the light curveRX J0513-69 � V Sge　(galactic SSS)SN Ia : initial and final state of binarySymbiotic channel in SD scenarioSSS channel in SD scenarioResponse of Accreting WDsNova & SN people need �more communication Starrfield et al. (2004) ApJ, 612,L53� “surface H burning” King et al. (2003) MNRAS, 341, L35�A new evolutionary channel for type Ia SN　“Dwarf nova causes steady H-burning”However, H does not ignite during dwarf nova outburst papers adopted King et al.’ ideaWDs evolve along with “steady burning zone” ?overproduction problem of SSSThank you